Manifestation of strong atmospheric phenomena in geophysical fields

A brief description of the geomorphological, historical, and archaeological aspects of the Colli Albani area, where the volcanic lakes of Albano and Nemi are situated, is followed by an examination on the problem of the policies of lake Albano regulation, by means of an ancient tunnel dating at least to the 5th century BC. In particular, it is investigated how, in the presence of even severe atmospheric phenomena, it was possible to control fluctuations in the level of the lake on the banks of which there were large settlements. Mathematical model simulations indicate the effectiveness of the ancient tunnel in achieving these objectives.

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Meteorological Characteristics of Energetic Atmospheric Phenomena

Physics of Particles and Nuclei Letters ◽

10.1134/s1547477120060102 ◽

2020 ◽

Vol 17 (6) ◽

pp. 840-847 ◽

Cited By ~ 1

Author(s):

E. K. Svechnikova ◽

N. V. Ilin ◽

E. A. Mareev

Keyword(s):

Atmospheric Phenomena

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Analysis of the Long-Term Trend of Temperature, Precipitation, and Dominant Atmospheric Phenomena in Lake Urmia

10.1007/698_2021_740 ◽

2021 ◽

Author(s):

Parvin Ghafarian ◽

Sahar Tajbakhsh ◽

Amir H. Delju

Keyword(s):

Lake Urmia ◽

Term Trend ◽

Atmospheric Phenomena ◽

Long Term Trend

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Solar structure and evolution

Living Reviews in Solar Physics ◽

10.1007/s41116-020-00028-3 ◽

2021 ◽

Vol 18 (1) ◽

Author(s):

Jørgen Christensen-Dalsgaard

Keyword(s):

Solar Surface ◽

Solar Neutrinos ◽

Solar Interior ◽

Stellar Structure ◽

The Sun ◽

Physical Processes ◽

Solar Evolution ◽

Internal Properties ◽

Atmospheric Phenomena

AbstractThe Sun provides a critical benchmark for the general study of stellar structure and evolution. Also, knowledge about the internal properties of the Sun is important for the understanding of solar atmospheric phenomena, including the solar magnetic cycle. Here I provide a brief overview of the theory of stellar structure and evolution, including the physical processes and parameters that are involved. This is followed by a discussion of solar evolution, extending from the birth to the latest stages. As a background for the interpretation of observations related to the solar interior I provide a rather extensive analysis of the sensitivity of solar models to the assumptions underlying their calculation. I then discuss the detailed information about the solar interior that has become available through helioseismic investigations and the detection of solar neutrinos, with further constraints provided by the observed abundances of the lightest elements. Revisions in the determination of the solar surface abundances have led to increased discrepancies, discussed in some detail, between the observational inferences and solar models. I finally briefly address the relation of the Sun to other similar stars and the prospects for asteroseismic investigations of stellar structure and evolution.

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